The real-time stellar evolution of Sakurai's object

Marcin Hajduk; Albert A. Zijlstra; Falk Herwig; Peter A M van Hoof; Florian Kerber; Stefan Kimeswenger; Don L Pollacco; Aneurin Evans; José A Lopéz; Myfanwy Bryce; Stewart P S Eyres; Mikako Matsuura

doi:10.1126/science.1108953

The real-time stellar evolution of Sakurai's object

Marcin Hajduk, Albert A. Zijlstra, Falk Herwig, Peter A M van Hoof, Florian Kerber, Stefan Kimeswenger, Don L Pollacco, Aneurin Evans, José A Lopéz, Myfanwy Bryce, Stewart P S Eyres, Mikako Matsuura

Faculty of Computing, Engineering and Science

Research output: Contribution to journal › Article › peer-review

Abstract

After a hot white dwarf ceases its nuclear burning, its helium may briefly and explosively reignite. This causes the star to evolve back into a cool giant, whereupon it experiences renewed mass ejection before reheating. A reignition event of this kind was observed in 1996 in V4334 Sgr (Sakurai's object). Its temperature decrease was 100 times the predicted rate. To understand its unexpectedly fast evolution, we have developed a model in which convective mixing is strongly suppressed under the influence of flash burning. The model predicts equally rapid reheating of the star. Radio emission from freshly ionized matter now shows that this reheating has begun. Such events may be an important source of carbon and carbonaceous dust in the Galaxy.

Original language	English
Pages (from-to)	231-3
Number of pages	3
Journal	Science
Volume	308
Issue number	5719
DOIs	https://doi.org/10.1126/science.1108953
Publication status	Published - 8 Apr 2005

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title = "The real-time stellar evolution of Sakurai's object",

abstract = "After a hot white dwarf ceases its nuclear burning, its helium may briefly and explosively reignite. This causes the star to evolve back into a cool giant, whereupon it experiences renewed mass ejection before reheating. A reignition event of this kind was observed in 1996 in V4334 Sgr (Sakurai's object). Its temperature decrease was 100 times the predicted rate. To understand its unexpectedly fast evolution, we have developed a model in which convective mixing is strongly suppressed under the influence of flash burning. The model predicts equally rapid reheating of the star. Radio emission from freshly ionized matter now shows that this reheating has begun. Such events may be an important source of carbon and carbonaceous dust in the Galaxy.",

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AU - Hajduk, Marcin

AU - Zijlstra, Albert A.

AU - Herwig, Falk

AU - van Hoof, Peter A M

AU - Kerber, Florian

AU - Kimeswenger, Stefan

AU - Pollacco, Don L

AU - Evans, Aneurin

AU - Lopéz, José A

AU - Bryce, Myfanwy

AU - Eyres, Stewart P S

AU - Matsuura, Mikako

PY - 2005/4/8

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AB - After a hot white dwarf ceases its nuclear burning, its helium may briefly and explosively reignite. This causes the star to evolve back into a cool giant, whereupon it experiences renewed mass ejection before reheating. A reignition event of this kind was observed in 1996 in V4334 Sgr (Sakurai's object). Its temperature decrease was 100 times the predicted rate. To understand its unexpectedly fast evolution, we have developed a model in which convective mixing is strongly suppressed under the influence of flash burning. The model predicts equally rapid reheating of the star. Radio emission from freshly ionized matter now shows that this reheating has begun. Such events may be an important source of carbon and carbonaceous dust in the Galaxy.

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DO - 10.1126/science.1108953

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JO - Science

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The real-time stellar evolution of Sakurai's object

Abstract

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